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SEEDS プロジェクトによる トランジット惑星系の直接撮像観測

SEEDS プロジェクトによる トランジット惑星系の直接撮像観測. 成田憲保 ( 国立天文台 ) 、 高橋安大 ( 東大 ) 、 佐藤文衛 ( 東工大 ) 、 鈴木竜二、神鳥亮、田村元秀 ( 国立天文台 ) 、 ほか SEEDS/ HiCIAO /AO188 チーム. Various Migration Models. consider gravitational interaction between disk-planet (disk-planet interaction models) e.g., Ida & Lin papers

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SEEDS プロジェクトによる トランジット惑星系の直接撮像観測

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  1. SEEDSプロジェクトによるトランジット惑星系の直接撮像観測SEEDSプロジェクトによるトランジット惑星系の直接撮像観測 成田憲保(国立天文台)、高橋安大(東大)、 佐藤文衛(東工大)、鈴木竜二、神鳥亮、田村元秀(国立天文台)、 ほか SEEDS/HiCIAO/AO188チーム

  2. Various Migration Models • consider gravitational interaction between • disk-planet (disk-planet interaction models) • e.g., Ida & Lin papers • planet-planet (planet-planet scattering models) • e.g., Chatterjee et al. 2008, Nagasawa et al. 2008 • planet-binary companion (Kozaimigration) • e.g., Wu & Murray 2003, Fabrycky & Tremaine 2007 • How can we discriminate those models by observations?

  3. Diagnostics to discriminate migration models small eccentricity and obliquity disk-planet interaction orbital eccentricity by radial velocity spin-orbit alignment angle by the RM effect • large eccentricity or obliquity • planet-planet scattering • Kozai migration

  4. Two Models Need Outer Massive Body captured planets orbit 1: low eccentricity and high inclination outer planet/BD ejected planet/BD orbit 2: high eccentricity and low inclination star binary orbital plane companion

  5. Can we discriminate two models? • Planet-Planet scattering Additional information from direct imaging! • Kozai migration Search for outer massive bodies is important to constrain migration mechanisms for each system

  6. SEEDS-RV Sub-category • Members: N. Narita, Y. Takahashi, B. Sato, R. Suzuki • Targets: Known planetary systems such as, • Very famous systems • long-term RV trend systems • Giant systems • Eccentric planetary systems • Transiting planetary systems (including eccentric/tilted systems) • 25+ systems observed • including 10+ transiting planetary systems (1st epoch) • some follow-up targets were observed (2nd epoch)

  7. 9 Results at a Glance

  8. First/Second Year Results • 9 out of 10 systems have companion candidates • high frequency of detecting candidate companions • Caution: this is only 1 epoch -> follow-up needed • Message to transit/secondary eclipse observers • Be careful about contamination of candidate companions, even they are not real binary companions • sometimes they may affect your results • 2nd epoch observations are ongoing • We can discriminate a migration mechanism for each target

  9. HAT-P-7 has a CPM Companion 2011 August K band 2009 August H band: NN et al. (2010) We have obtained J, H, Ks, L’ band images to determine spectral type

  10. HAT-P-11 (1st epoch) Several companion candidates detected

  11. HAT-P-11 (2nd epoch) BUT they did not pass the common proper motion test!

  12. Conclusions • Direct imaging for known planetary systems is important • We can constrain migration mechanism for each system • We found high frequency of detecting candidate companions • Caution: this is only 1 epoch • Further follow-up observations are important • Be careful for contamination of companion candidates • Depth of transit/secondary eclipse may be affected, even they are not real companions

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